DOCSLIB.ORG

March 21–25, 2016

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, Lunar and Planetary Institute Fred Hörz, NASA Johnson Space Center Virgil Sharpton, Lunar and Planetary Institute Kristen John, NASA Johnson Space Center Christine Shupla, Lunar and Planetary Institute Georgiana Kramer, Lunar and Planetary Institute Bradley Thomson, Boston University Tom Lapen, University of Houston Melissa Trainer, NASA Goddard Space Flight Center Samuel Lawrence, Arizona State University Jennifer Whitten, Smithsonian Institution Produced by the Lunar and Planetary Institute (LPI), 3600 Bay Area Boulevard, Houston TX 77058-1113, which is supported by NASA under Award No. NNX15AL12A. Logistics, administrative, and publications support for the conference were provided by USRA Houston Meeting Planning Services. ABOUT LPSC The Lunar and Planetary Science Conference brings together international specialists in petrology, geochemistry, geophysics, geology, and astronomy to present the latest results of research in planetary science. The four and a half-day conference is organized by topical symposia and problem-oriented sessions. LOGISTICAL INFORMATION Venue Address and Phone Number The conference is being held at The Woodlands Waterway Marriott Hotel and Convention Center, 1601 Lake Robbins Dr., The Woodlands TX 77380. LPSC conference staff can be reached by calling the hotel at 281-367-9797 and asking for the conference registration desk. Please note that copy and printing services are not available at the conference registration desk, and must be arranged through the hotel business center. For your convenience, a minimal number of laptops and printers will be available in the Wi-Fi access rooms (see below). Registration Conference registration and check-in will be held on Sunday from 4:00 to 8:00 p.m., from 8:00 a.m. to 5:00 p.m. Monday through Thursday, and from 8:00 to 10:00 a.m. Friday. Conference badges provide access to all technical sessions, special events, and shuttle service. Speaker-Ready Room/Presentation Check-In Presentation validation will be in the Alden Bridge Room. Those presenting on Monday morning should check in their presentations on Sunday evening when they register. Hours of Operation: Sunday, 4:00–8:00 p.m.; Monday– Thursday, 7:00 a.m.–5:30 p.m.; and Friday, 7:00–10:00 a.m. Internet Access Complimentary Wi-Fi service will be available throughout the duration of the conference in selected public areas, including the Town Center Exhibit Area and immediate vicinity. As in previous years, Wi-Fi service will NOT be available in the oral session rooms for anyone other than the selected LPSC microbloggers. This restriction is (and has been) in place to curtail activities that could be distracting to speakers during their presentations. Conference Shuttle Service Conference shuttle bus service between the venue and the approved list of hotels will be provided on Sunday evening during the registration time and throughout the duration of the conference. Shuttle service will run before and immediately following all technical sessions. Detailed shuttle schedules are available in the registration area and on the LPSC website at www.hou.usra.edu/meetings/lpsc2016/travel/shuttleInfo. Poster Printing Available AlphaGraphics will have a staffed booth at The Woodlands Waterway Marriott, just outside the Town Center Exhibit Area on the first floor. Poster presenters can pick up pre-ordered posters or place orders for posters beginning on Sunday, March 20. For more information, visit their website at www.txagprinting.com. Personal Schedule Create your own personal meeting schedule using the Personal Schedule tool found in the USRA Meeting Portal at https://www.hou.usra.edu/meeting_portal/schedule/. Select the sessions you want to attend or talks you want to hear, then create a shareable schedule that can be viewed on your smart phone or shared with a colleague. LIST OF EXHIBITORS ADS/Smithsonian Astrogeology Science Center, Astrophysical Observatory U.S. Geological Survey 60 Garden Street 2255 North Gemini Drive Cambridge MA 02138 Flagstaff AZ 86001 Contact: Donna Thompson Contact: Trent Hare [email protected] [email protected] The NASA Astrophysics Data System (ADS) is a Digital The United States Geological Survey’s Astrogeology Library portal containing the journal literature of astronomy Science Center (USGS-ASC), located in Flagstaff, Arizona, and physics (including geophysics). Our new interface has provides support to the planetary community with unique some exciting new features that streamline your searching inhouse and online resources and tools to help researchers of our extensive database. Come and see some new accomplish their science objectives. The USGS-ASC searching techniques. Learn how to use ADS to populate conducts innovative research and develops state-of-the-art your ORCiD profile. Even if you’ve used ADS in the past, software and techniques that advance the fields of stop by and see our new search engine, network planetary geosciences, remote sensing, and cartography. visualizations, and metrics summary. The USGS-ASC also establishes mapping and archiving standards and supports the distribution of map and Arecibo Observatory data products. www.naic.edu HC3 Box 53995 ASU Education Through eXploration Arecibo PR 00612 (ETX Center) www.etx.io/ Contact: Linda Rodriguez-Ford ASU Tempe Campus School of Earth and Space [email protected] Exploration Bateman Physical Sciences, F-Wing, Room 686 Located in Puerto Rico, the Arecibo Observatory is home Tempe AZ 85287-1404 to the largest and most sensitive single dish radio telescope in the world. It is an NSF facility managed under Contact: Leon Manfredi a cooperative agreement by SRI International, Universities [email protected] Space Research Association, and Universidad Metropolitana. The Arecibo Planetary Radar program is The ASU Center for Education Through eXploration (ETX supported by NASA’s Near Earth Object Observation Center) advances a new educational philosophy that program. AO’s planetary radar system is the world’s most centers teaching and learning on open, transdisciplinary powerful instrument for post-discovery characterization and questions rather than simply mastering what is known. We orbital refinement of near-Earth objects. call this philosophy “Education Through eXploration” (ETX) and are developing and deploying digital learning products and platforms that advance this philosophy engagingly, adaptively, and at scale as part of a new NASA education initiative of the School of Earth and Space Exploration. Brown University DEEPS e‐Mars Team Web Application: MarsSI www.brown.edu/academics/earth-environmental-planetary- Laboratoire de Géologie de Lyon Bâtiment Géode sciences/ 2 Rue Raphaël Dubois 324 Brook Street Villeurbanne 69622 France Providence RI 02912 Contact: Loïc Lozaćh Contact: Daniel Moriarty III [email protected] [email protected] MarsSI (Acronym of MARS System of Information) is a web Our graduate program is rated among the top programs in geographic information system application that allows the the nation and the world. Our faculty members, nationally managing and processing of martian orbital data. From this and internationally acknowledged leaders in their fields, application, users are able to easily and rapidly select engage in externally supported research that is defining the observations, process raw data via proposed automatic direction of inquiry for the next decade. pipelines, and get back ready-to-use data for science. Also, MarsSI proposes automatic stereo-restitution pipelines to Cambridge University Press produce digital terrain models (DTM) from CTX and HIRISE stereo pairs. www.cambridge.org/us/academic 32 Avenue of the Americas New York NY 10013 Fibertek, Inc. fibertek.com Contact: Emma Kiddle 13605 Dulles Technology Drive [email protected] Herndon VA 20171 Cambridge’s publishing in books and journals combines Contact: Mark Storm state-of-the-art content with the highest standards of [email protected] scholarship, writing, and production. Visit
Recommended publications
  • Aitken Basin

    Aitken Basin

    Geological and geochemical analysis of units in the South Pole – Aitken Basin A.M. Borst¹,², F.S. Bexkens¹,², B. H. Foing², D. Koschny² ¹ Department of Petrology, VU University Amsterdam ² SCI-S. Research and Scientific Support Department, ESA – ESTEC Student Planetary Workshop 10-10-2008 ESA/ESTEC The Netherlands The South Pole – Aitken Basin Largest and oldest Lunar impact basin - Diameter > 2500 km - Depth > 12 km - Age 4.2 - 3.9 Ga Formed during Late heavy bombardment? Window into the interior and evolution of the Moon Priority target for future sample return missions Digital Elevation Model from Clementine altimetry data. Produced in ENVI, 50x vertical exaggeration, orthographic projection centered on the far side. Red +10 km, purple/black -10km. (A.M.Borst et.al. 2008) 1 The Moon and the SPA Basin Geochemistry Iron map South Pole – Aitken Basin mafic anomaly • High Fe, Th, Ti and Mg abundances • Excavation of mafic deep crustal / upper mantle material Thorium map Clementine 750 nm albedo map from USGS From Paul Lucey, J. Geophys. Res., 2000 Map-a-Planet What can we learn from the SPA Basin? • Large impacts; Implications and processes • Volcanism; Origin, age and difference with near side mare basalts • Cratering record; Age, frequency and size distribution • Late Heavy Bombardment; Intensity, duration and origin • Composition of the deeper crust and possibly upper mantle 2 Topics of SPA Basin study 1) Global structure of the basin (F.S. Bexkens et al, 2008) • Rims, rings, ejecta distribution, subsequent craters modifications, reconstructive
  • Minutes of the January 25, 2010, Meeting of the Board of Regents

    Minutes of the January 25, 2010, Meeting of the Board of Regents

    MINUTES OF THE JANUARY 25, 2010, MEETING OF THE BOARD OF REGENTS ATTENDANCE This scheduled meeting of the Board of Regents was held on Monday, January 25, 2010, in the Regents’ Room of the Smithsonian Institution Castle. The meeting included morning, afternoon, and executive sessions. Board Chair Patricia Q. Stonesifer called the meeting to order at 8:31 a.m. Also present were: The Chief Justice 1 Sam Johnson 4 John W. McCarter Jr. Christopher J. Dodd Shirley Ann Jackson David M. Rubenstein France Córdova 2 Robert P. Kogod Roger W. Sant Phillip Frost 3 Doris Matsui Alan G. Spoon 1 Paul Neely, Smithsonian National Board Chair David Silfen, Regents’ Investment Committee Chair 2 Vice President Joseph R. Biden, Senators Thad Cochran and Patrick J. Leahy, and Representative Xavier Becerra were unable to attend the meeting. Also present were: G. Wayne Clough, Secretary John Yahner, Speechwriter to the Secretary Patricia L. Bartlett, Chief of Staff to the Jeffrey P. Minear, Counselor to the Chief Justice Secretary T.A. Hawks, Assistant to Senator Cochran Amy Chen, Chief Investment Officer Colin McGinnis, Assistant to Senator Dodd Virginia B. Clark, Director of External Affairs Kevin McDonald, Assistant to Senator Leahy Barbara Feininger, Senior Writer‐Editor for the Melody Gonzales, Assistant to Congressman Office of the Regents Becerra Grace L. Jaeger, Program Officer for the Office David Heil, Assistant to Congressman Johnson of the Regents Julie Eddy, Assistant to Congresswoman Matsui Richard Kurin, Under Secretary for History, Francisco Dallmeier, Head of the National Art, and Culture Zoological Park’s Center for Conservation John K.
  • Alaska Regional Directors Offices Director Email Address Contact Numbers Supt

    Alaska Regional Directors Offices Director Email Address Contact Numbers Supt

    Alaska Regional Directors Offices Director Email Address Contact Numbers Supt. Phone Fax Code ABLI RegionType Unit U.S Fish and Wildlife Service (FWS) Alaska Region (FWS) HASKETT,GEOFFREY [email protected] 1011 East Tudor Road Phone: 907‐ 786‐3309 Anchorage, AK 99503 Fax: 907‐ 786‐3495 Naitonal Park Service(NPS) Alaska Region (NPS) MASICA,SUE [email protected] 240 West 5th Avenue,Suite 114 Phone:907‐644‐3510 Anchoorage,AK 99501 Bureau of Indian Affairs(BIA) Alaska Region (BIA) VIRDEN,EUGENE [email protected] Bureau of Indian Affairs Phone: 907‐586‐7177 PO Box 25520 Telefax: 907‐586‐7252 709 West 9th Street Juneau, AK 99802 Anchorage Agency Phone: 1‐800‐645‐8465 Bureau of Indian Affairs Telefax:907 271‐4477 3601 C Street Suite 1100 Anchorage, AK 99503‐5947 Telephone: 1‐800‐645‐8465 Bureau of Land Manangement (BLM) Alaska State Office (BLM) CRIBLEY,BUD [email protected] Alaska State Office Phone: 907‐271‐5960 222 W 7th Avenue #13 FAX: 907‐271‐3684 Anchorage, AK 99513 United States Geological Survey(USGS) Alaska Area (USGS) BARTELS,LESLIE lholland‐[email protected] 4210 University Dr., Anchorage, AK 99508‐4626 Phone:907‐786‐7055 Fax: 907‐ 786‐7040 Bureau of Ocean Energy Management(BOEM) Alaska Region (BOEM) KENDALL,JAMES [email protected] 3801 Centerpoint Drive Phone: 907‐ 334‐5208 Suite 500 Anchorage, AK 99503 Ralph Moore [email protected] c/o Katmai NP&P (907) 246‐2116 ANIA ANTI AKR NPRES ANIAKCHAK P.O. Box 7 King Salmon, AK 99613 (907) 246‐3305 (907) 246‐2120 Jeanette Pomrenke [email protected] P.O.
  • 1922 Elizabeth T

    1922 Elizabeth T

    co.rYRIG HT, 192' The Moootainetro !scot1oror,d The MOUNTAINEER VOLUME FIFTEEN Number One D EC E M BER 15, 1 9 2 2 ffiount Adams, ffiount St. Helens and the (!oat Rocks I ncoq)Ora,tecl 1913 Organized 190!i EDITORlAL ST AitF 1922 Elizabeth T. Kirk,vood, Eclttor Margaret W. Hazard, Associate Editor· Fairman B. L�e, Publication Manager Arthur L. Loveless Effie L. Chapman Subsc1·iption Price. $2.00 per year. Annual ·(onl�') Se,·ent�·-Five Cents. Published by The Mountaineers lncorJ,orated Seattle, Washington Enlerecl as second-class matter December 15, 19t0. at the Post Office . at . eattle, "\Yash., under the .-\0t of March 3. 1879. .... I MOUNT ADAMS lllobcl Furrs AND REFLEC'rION POOL .. <§rtttings from Aristibes (. Jhoutribes Author of "ll3ith the <6obs on lltount ®l!!mµus" �. • � J� �·,,. ., .. e,..:,L....._d.L.. F_,,,.... cL.. ��-_, _..__ f.. pt",- 1-� r�._ '-';a_ ..ll.-�· t'� 1- tt.. �ti.. ..._.._....L- -.L.--e-- a';. ��c..L. 41- �. C4v(, � � �·,,-- �JL.,�f w/U. J/,--«---fi:( -A- -tr·�� �, : 'JJ! -, Y .,..._, e� .,...,____,� � � t-..__., ,..._ -u..,·,- .,..,_, ;-:.. � --r J /-e,-i L,J i-.,( '"'; 1..........,.- e..r- ,';z__ /-t.-.--,r� ;.,-.,.....__ � � ..-...,.,-<. ,.,.f--· :tL. ��- ''F.....- ,',L � .,.__ � 'f- f-� --"- ��7 � �. � �;')'... f ><- -a.c__ c/ � r v-f'.fl,'7'71.. I /!,,-e..-,K-// ,l...,"4/YL... t:l,._ c.J.� J..,_-...A 'f ',y-r/� �- lL.. ��•-/IC,/ ,V l j I '/ ;· , CONTENTS i Page Greetings .......................................................................tlristicles }!}, Phoiitricles ........ r The Mount Adams, Mount St. Helens, and the Goat Rocks Outing .......................................... B1/.ith Page Bennett 9 1 Selected References from Preceding Mount Adams and Mount St.
  • Ahuna Mons on Ceres 29 July 2019

    Ahuna Mons on Ceres 29 July 2019

    Image: Ahuna Mons on Ceres 29 July 2019 More recently, a study of Dawn data led by ESA research fellow Ottaviano Ruesch and Antonio Genova (Sapienza Università di Roma), published in Nature Geoscience in June, suggests that a briny, muddy 'slurry' exists below Ceres' surface, surging upwards towards and through the crust to create Ahuna Mons. Another recent study, led by Javier Ruiz of Universidad Complutense de Madrid and published in Nature Astronomy in July, also indicates that the dwarf planet has a surprisingly dynamic geology. Ceres was also the focus of an earlier study by Credit: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA ESA's Herschel space observatory, which detected water vapour around the dwarf planet. Published in Nature in 2014, the result provided a strong indication that Ceres has ice on or near its surface. This image, based on observations from NASA's Dawn confirmed Ceres' icy crust via direct Dawn spacecraft, shows the largest mountain on observation in 2016, however, the contribution of the dwarf planet Ceres. the ice deposits to Ceres' exosphere turned out to be much lower than that inferred from the Herschel Dawn was the first mission to orbit an object in the observations. asteroid belt between Mars and Jupiter, and spent time at both large asteroid Vesta and dwarf planet The perspective view depicted in this image uses Ceres. Ceres is one of just five recognised dwarf enhanced-color combined images taken using blue planets in the Solar System (Pluto being another). (440 nm), green (750 nm), and infrared (960 nm) Dawn entered orbit around this rocky world on 6 filters, with a resolution of 35 m/pixel.
  • Small, Young Volcanic Deposits Around the Lunar Farside Craters Rosseland, Bolyai, and Roche

    Small, Young Volcanic Deposits Around the Lunar Farside Craters Rosseland, Bolyai, and Roche

    44th Lunar and Planetary Science Conference (2013) 2024.pdf SMALL, YOUNG VOLCANIC DEPOSITS AROUND THE LUNAR FARSIDE CRATERS ROSSELAND, BOLYAI, AND ROCHE. J. H. Pasckert1, H. Hiesinger1, and C. H. van der Bogert1. 1Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany. jhpasckert@uni- muenster.de Introduction: To understand the thermal evolu- mare basalts on the near- and farside. This gives us the tion of the Moon it is essential to investigate the vol- opportunity to investigate the history of small scale canic history of both the lunar near- and farside. While volcanism on the lunar farside. the lunar nearside is dominated by mare volcanism, the farside shows only some isolated mare deposits in the large craters and basins, like the South Pole-Aitken basin or Tsiolkovsky crater [e.g., 1-4]. This big differ- ence in volcanic activity between the near- and farside is of crucial importance for understanding the volcanic evolution of the Moon. The extensive mare volcanism of the lunar nearside has already been studied in great detail by numerous authors [e.g., 4-8] on the basis of Lunar Orbiter and Apollo data. New high-resolution data obtained by the Lunar Reconnaissance Orbiter (LRO) and the SELENE Terrain Camera (TC) now allow us to investigate the lunar farside in great detail. Basaltic volcanism of the lunar nearside was active for almost 3 Ga, lasting from ~3.9-4.0 Ga to ~1.2 Ga before present [5]. In contrast to the nearside, most eruptions of mare deposits on the lunar farside stopped much earlier, ~3.0 Ga ago [9].
  • Thickness of the Martian Crust: Improved Constraints from Geoid-To-Topography Ratios Mark A

    Thickness of the Martian Crust: Improved Constraints from Geoid-To-Topography Ratios Mark A

    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109, E01009, doi:10.1029/2003JE002153, 2004 Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios Mark A. Wieczorek De´partement de Ge´ophysique Spatiale et Plane´taire, Institut de Physique du Globe de Paris, Saint-Maur, France Maria T. Zuber Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA Received 10 July 2003; revised 1 September 2003; accepted 24 November 2003; published 24 January 2004. [1] The average crustal thickness of the southern highlands of Mars was investigated by calculating geoid-to-topography ratios (GTRs) and interpreting these in terms of an Airy compensation model appropriate for a spherical planet. We show that (1) if GTRs were interpreted in terms of a Cartesian model, the recovered crustal thickness would be underestimated by a few tens of kilometers, and (2) the global geoid and topography signals associated with the loading and flexure of the Tharsis province must be removed before undertaking such a spatial analysis. Assuming a conservative range of crustal densities (2700–3100 kg mÀ3), we constrain the average thickness of the Martian crust to lie between 33 and 81 km (or 57 ± 24 km). When combined with complementary estimates based on crustal thickness modeling, gravity/topography admittance modeling, viscous relaxation considerations, and geochemical mass balance modeling, we find that a crustal thickness between 38 and 62 km (or 50 ± 12 km) is consistent with all studies. Isotopic investigations based on Hf-W and Sm-Nd systematics suggest that Mars underwent a major silicate differentiation event early in its evolution (within the first 30 Ma) that gave rise to an ‘‘enriched’’ crust that has since remained isotopically isolated from the ‘‘depleted’’ mantle.
  • New Studies Provide Unexpected Insights Into Dwarf Planet Ceres 1 September 2016

    New Studies Provide Unexpected Insights Into Dwarf Planet Ceres 1 September 2016

    New studies provide unexpected insights into dwarf planet Ceres 1 September 2016 Mons. The dome-shaped mountain has an elliptical base and a concave top, as well as other properties that indicate cryovolcanism. The authors applied models to determine the age of Ahuna Mons, finding it to have formed after the craters surrounding it, which suggests that it came into existence relatively recently. There is no evidence for compressional tectonism, nor for erosional features, the authors say; it appears that extrusion is a main driver behind the formation of Ahuna Mons. Although the exact material driving the cryovolcano cannot be determined without further data, the authors propose that chlorine salts, which have been previously detected in a different region of Ceres, could have been present with water ice below Ceres' surface and driven the chemical activity that formed Ahuna Mons. In a second study, Jean-Philippe Combe et al. A high resolution Dawn framing camera image of Ahuna describe the detection of water ice - exposed on the Mons. Image width is 30 km. Credit: NASA/JPL- surface of Ceres. The dwarf planet was known to Caltech/UCLA/MPS/DLR/IDA contain water ice, but water ice is also expected to be unstable on its surface, so scientists were unsure whether it could be detected there. They used the Visible and InfraRed (VIR) mapping Six studies published today in Science highlight spectrometer onboard the Dawn spacecraft to new and unexpected insights into Ceres, a dwarf analyze a highly reflective zone in a young crater planet and the largest object in the asteroid belt called Oxo, on five occasions during 2015.
  • (704) Interamnia from Its Occultations and Lightcurves

    (704) Interamnia from Its Occultations and Lightcurves

    International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum.
  • Impact Melt Emplacement on Mercury

    Impact Melt Emplacement on Mercury

    Western University Scholarship@Western Electronic Thesis and Dissertation Repository 7-24-2018 2:00 PM Impact Melt Emplacement on Mercury Jeffrey Daniels The University of Western Ontario Supervisor Neish, Catherine D. The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Jeffrey Daniels 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons, Physical Processes Commons, and the The Sun and the Solar System Commons Recommended Citation Daniels, Jeffrey, "Impact Melt Emplacement on Mercury" (2018). Electronic Thesis and Dissertation Repository. 5657. https://ir.lib.uwo.ca/etd/5657 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract Impact cratering is an abrupt, spectacular process that occurs on any world with a solid surface. On Earth, these craters are easily eroded or destroyed through endogenic processes. The Moon and Mercury, however, lack a significant atmosphere, meaning craters on these worlds remain intact longer, geologically. In this thesis, remote-sensing techniques were used to investigate impact melt emplacement about Mercury’s fresh, complex craters. For complex lunar craters, impact melt is preferentially ejected from the lowest rim elevation, implying topographic control. On Venus, impact melt is preferentially ejected downrange from the impact site, implying impactor-direction control. Mercury, despite its heavily-cratered surface, trends more like Venus than like the Moon.
  • DMAAC – February 1973

    DMAAC – February 1973

    LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base.
  • Hi-Resolution Map Sheet

    Hi-Resolution Map Sheet

    Controlled Mosaic of Enceladus Hamah Sulci Se 400K 43.5/315 CMN, 2018 GENERAL NOTES 66° 360° West This map sheet is the 5th of a 15-quadrangle series covering the entire surface of Enceladus at a 66° nominal scale of 1: 400 000. This map series is the third version of the Enceladus atlas and 1 270° West supersedes the release from 2010 . The source of map data was the Cassini imaging experiment (Porco et al., 2004)2. Cassini-Huygens is a joint NASA/ESA/ASI mission to explore the Saturnian 350° system. The Cassini spacecraft is the first spacecraft studying the Saturnian system of rings and 280° moons from orbit; it entered Saturnian orbit on July 1st, 2004. The Cassini orbiter has 12 instruments. One of them is the Cassini Imaging Science Subsystem 340° (ISS), consisting of two framing cameras. The narrow angle camera is a reflecting telescope with 290° a focal length of 2000 mm and a field of view of 0.35 degrees. The wide angle camera is a refractor Samad with a focal length of 200 mm and a field of view of 3.5 degrees. Each camera is equipped with a 330° 300° large number of spectral filters which, taken together, span the electromagnetic spectrum from 0.2 60° 320° 310° to 1.1 micrometers. At the heart of each camera is a charged coupled device (CCD) detector 60° consisting of a 1024 square array of pixels, each 12 microns on a side. MAP SHEET DESIGNATION Peri-Banu Se Enceladus (Saturnian satellite) 400K Scale 1 : 400 000 43.5/315 Center point in degrees consisting of latitude/west longitude CMN Controlled Mosaic with Nomenclature Duban 2018 Year of publication IMAGE PROCESSING3 Julnar Ahmad - Radiometric correction of the images - Creation of a dense tie point network 50° - Multiple least-square bundle adjustments 50° - Ortho-image mosaicking Yunan CONTROL For the Cassini mission, spacecraft position and camera pointing data are available in the form of SPICE kernels.